riken-ithems-report-21 impacts of jets and winds from
TRANSCRIPT
IPMU21-0080RIKEN-iTHEMS-Report-21
Impacts of Jets and Winds From Primordial Black Holes
Volodymyr Takhistov,1, ∗ Philip Lu,2, 3, † Kohta Murase,4, 5, ‡ Yoshiyuki Inoue,6, 7, 1, § and Graciela B. Gelmini2, ¶
1Kavli Institute for the Physics and Mathematics of the Universe (WPI), UTIASThe University of Tokyo, Kashiwa, Chiba 277-8583, Japan
2Department of Physics and Astronomy, University of California, Los AngelesLos Angeles, California, 90095-1547, USA
3Center for Theoretical Physics, Department of Physics and Astronomy, Seoul National University, Seoul 08826, Korea4Department of Physics; Department of Astronomy and Astrophysics; Center for Multimessenger Astrophysics,
The Pennsylvania State University, University Park, Pennsylvania 16802, USA5Center for Gravitational Physics, Yukawa Institute for Theoretical Physics, Kyoto, Kyoto 16802, Japan
6Department of Earth and Space Science, Graduate School of Science,Osaka University, Toyonaka, Osaka 560-0043, Japan
7Interdisciplinary Theoretical & Mathematical Science Program (iTHEMS),RIKEN, 2-1 Hirosawa, Saitama 351-0198, Japan
(Dated: November 17, 2021)
Primordial black holes (PBHs) formed in the early Universe constitute an attractive candidatefor dark matter. Within the gaseous environment of the interstellar medium, PBHs with accretiondisks naturally launch outflows such as winds and jets. PBHs with significant spin can sustainpowerful relativistic jets and generate associated cocoons. Jets and winds can efficiently deposittheir kinetic energies and heat the surrounding gas through shocks. Focusing on the Leo T dwarfgalaxy, we demonstrate that these considerations can provide novel tests of PBHs over a significant∼ 10−2M − 106M mass range, including the parameter space associated with gravitational waveobservations by the LIGO and VIRGO Collaborations. Observing the morphology of emission couldallow to distinguish between jet and wind contributions, and hence indirectly detect spinning PBHs.
I. INTRODUCTION
Primordial black holes (PBHs) that could have formedin the early Universe prior to galaxies and stars can con-stitute a significant fraction of the dark matter (DM),can significantly affect the cosmological history and havebeen associated with a variety of observational signa-tures (e.g., [1–34]). Depending on the formation scenario,the mass of PBHs can span many orders of magnitude.
Particularly intriguing are PBHs in the stellar BHmass range of ∼ 10 − 102M, which have been di-rectly linked with the breakthrough observations of grav-itational waves (GWs) by the LIGO and Virgo col-laborations (LVC) [35]. Dozens of binary BH mergersources have already been detected [36]. While uncer-tainties exist (e.g., [37, 38]), only a fraction fPBH .O(10−3) of PBHs contributing to the DM energy den-sity, fPBH = (ΩPBH/ΩDM), is needed to account for theGW data [12, 39–50].
The first detected intermediate mass BH, theGW190521 LVC event, with a total merger mass of∼ 150M that lies in the pair instability supernova massgap [51], has challenged conventional astrophysical in-terpretations. Further, GW candidate events consistentwith solar mass BHs, lying in the lower mass gap region
∗ [email protected]† [email protected]‡ [email protected]§ [email protected]¶ [email protected]
. 3M, have drawn speculations about possible non-astrophysical origins (e.g., [27, 28, 34, 52–59]).
While a variety of different constraints exist over the∼ 1 − 104M mass range for PBHs contributing signif-icantly to the DM abundance [60–69], stellar mass andintermediate mass PBHs have often been considered asnonrotating (Schwarzschild) BHs [70–72]. Recently, out-flow emission has been proposed as a new observable forstudying accreting nonrotating PBHs [67, 69].
PBHs can be formed with significant spin (KerrBHs) (e.g., [21–23, 29, 73–77]) as well as acquire spinvia accretion [78] or hierarchical mergers [79]. Asidefrom mass and charge, spin constitutes a fundamen-tal conserved BH parameter. Recent works focusing onsmall PBHs undergoing efficient Hawking evaporationhave shown that spin can significantly affect observa-tions (e.g., [9, 80–88]).
In this work we analyze effects of outflow emissionsfrom PBHs on the surrounding interstellar medium(ISM) gas for stellar and intermediate mass PBHs. Spin-ning PBHs can support powerful relativistic jets, an im-portant emission component that has been previously un-derexplored. We revisit emission from winds associatedwith accreting PBHs, which could be highly efficient. Aswe demonstrate, these combined effects allow for strin-gent tests of PBHs over a significant parameter space.
II. ACCRETION DISK EMISSION
As PBHs traverse the ISM, they interact with thesurrounding gas, depositing energy and heat. This
arX
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111.
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[as
tro-
ph.H
E]
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Nov
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1
2
10−1 100 101 102 103 104 105 106
M (M)
1021
1024
1027
1030
1033
1036
1039
1042
1045H
(erg
/s)
FIG. 1. Comparison between the spin a = 0 (dashed) andspin a = 0.9 (solid) cases of the effective gas heating from var-ious contributions, bremsstrahlung (magenta), inverse Comp-ton (red) and dynamical friction (green).
has been recently analyzed in detail for SchwarzschildPBHs [67, 69]. We discuss how the PBH spin affectsaccretion disk emission. We take the convention c = 1.
In the presence of non-negligible spin, the radius of thePBH innermost stable circular orbit (ISCO) that maymark the inner edge of the accretion disk is [89]
rmin = GM(
3 + Z2 ∓ [(3− Z1)(3 + Z1 + 2Z2)]1/2),
(1)where
Z1 ≡ 1 +(
1− χ2)1/3[(
1 + χ)1/3
+(
1− χ)1/3]
Z2 ≡(
3χ2 + Z21
)1/2. (2)
Here M is the PBH mass, χ = 2a/Rs, a is spin Kerrparameter, and Rs = 2GM is the Schwarzschild radius,where natural units are adopted.
To estimate the change in PBH emission with spin, wefocus on the radiatively inefficient accretion flows (RI-AFs) that form when the accretion is sub-Eddington [90],as relevant for our parameter space of interest [67,69]. We follow the approximate analytic expressionsof Ref. [91] to describe the complex multiblackbodyRIAF spectrum, employing updated phenomenologicalinput parameters describing emission, as in the analy-sis for Schwarzschild PBHs [67, 69]. With respect toRefs. [67, 69] the components are modified through non-trivial functions of temperature as well as other inputsdependent on rmin.
Photons emitted from the accretion disk interact withand heat the surrounding ISM. The Bondi-Hoyle accre-
tion rate is [92–94]
M = 4πr2B vρa = 4πG2M2nµmp
v3
' 2.3× 1031 erg/s(
M
1 M
)2
×( n
0.07 cm−3
)( v
10 km/s
)−3, (3)
where rB = 2GM/v2 is the Bondi radius, ρa is the am-bient gas density, µ is the mean molecular weight, nis the ISM gas number density, mp is the proton massand v ≡ (v2 + c2s)1/2. Here v is the PBH velocity rela-tive to the ISM gas and cs is the temperature-dependentsound speed in gas, which we take to be approximatelycs ∼ 10 km/s [63].
Favorable systems, such as the dwarf galaxy Leo T,are rich in atomic hydrogen gas that strongly absorbsionizing radiation, E & Ei = 13.6eV. However, atomichydrogen is optically thin both below the Ei thresh-old and for hard X-rays E & 1keV. We consider thephoto-ionization cross section [95, 96] to be σ(E) =σ0y− 3
2
(1 + y
12
)−4, where y = E/E0, E0 = 1/2Ei and
σ0 = 6.06 × 10−16 cm2. For energies above 30 eV, weuse the attenuation length data from Fig. (32.16) ofRef. [97], which includes the Thompson (Compton) scat-tering cross-section that is dominant for high energies.The optical depth is τ(n,E) = σ(E)nrsys, where rsys isthe characteristic size of the system. The heating rateis then a function of both the frequency-dependent lumi-nosity Lν and the optical depth, τ ,
Hpe(M,n, v) =∫ Emax
Ei
Lν(M,n, v)fh(1− e−τ
)dν , (4)
with an additional factor of fh ∼ 1/3 [98] for the fractionof energy loss deposited as heat. We integrate Eq. (4)up to the electron temperature Emax ∼ few × Te, abovewhich the emission falls off exponentially.
As shown by the semi-analytic modeling [91], the elec-tron temperature in the accretion disk is set by the bal-ance of heating and emission processes. Both viscousheating, which is dominant at low accretion rates, andion-electron collisional heating for higher accretion ratesscale approximately inversely with the ISCO radius rmin.We neglect the effects of collisionless heating in our treat-ment. Thus, assuming the disk and BH are aligned,higher PBH spins result in rmin moving inwards andgenerally increase the electron temperature of the diskplasma. In turn, increased emission from the three coun-terbalancing processes: synchrotron, inverse Compton(IC), and bremsstrahlung, resolves the temperature toa new higher equilibrium.
In Fig. 1, we display contributions to effective heatingfor Schwarzschild as well as spinning (a = 0.9) PBHs. Re-garding heat deposition by emission from the innermostregion around the ISCO, we find that spinning PBHs
3
yield an order of magnitude increase in the IC contri-bution, but not the synchotron (not displayed) or thebremsstrahlung emissions. The synchrotron and IC lu-minosity of RIAFs have Lsyn ∝ T 7
e and T 6+αICe for αIC .
1 (e.g., [99]), so the temperature dependence is strongerfor the synchrotron in general. For the bremsstrahlungspectrum, increasing the electron temperature does notsignificantly increase the luminosity throughout the spec-trum, but rather further extends it to higher frequencies.However, our hydrogen-rich environments of interest suchas the Leo T dwarf galaxy are optically thin to Comptonscattering at these high energies, so the extended spec-trum does not increase the deposited energy and heating.
Similarly, although the synchotron luminosity is oftendominant in RIAF disks, synchotron radiation predomi-nantly emits in radio and infrared frequencies that inter-act negligibly with atomic hydrogen. Hence, we do notconsider this contribution. The higher temperature ofspinning black holes does increase the synchrotron emis-sion and also shifts the synchotron peak to higher fre-quencies, closer to the ionization threshold of 13.6 eV.Photons from this synchotron peak provide targets forthe IC scattering. Thus, the augmented synchotron peaknearer to the ionization, along with more efficient IC up-scattering at higher temperatures, significantly booststhe quantity of strongly absorbed ionizing IC photons,leading to a non-linear rise in the heating rate. We notethat throughout we consider that emission follows a sin-gle zone model. However, significant uncertainties existand other models are also possible.
We also display in Fig. 1 dynamical friction, withheat generated by dynamical friction force Fdyn =−4πG2M2ρI/v2. Here I is a geometrical integral thatis only weakly affected by the ISCO/min radius throughan additive ln (rmax/rmin) contribution when v/cs > 1.Hence, the inclusion of PBH spin does not significantlyaffect this energy deposit component.
III. JETS AND COCOONS
In addition to emission from the accretion disk, spin-ning astrophysical BHs can naturally power collimatedrelativistic jets 1 via the electromagnetic extraction of ro-tational energy from a BH through the Blandford-Znajek(BZ) mechanism [102]. We now discuss the emission as-sociated with jets and related cocoons for highly spinning(a > 0.5) PBHs traversing the ISM.
With the strong magnetic fields relevant for jet launch-ing, numerical simulations indicate that “magnetically-arrested” disks (MADs) can be expected to form [103,
1 Under specific circumstances, the formation of jets via otherchannels, such as neutrino-antineutrino annihilation (e.g., [100])or magnetocentrifugal force through the disk magnetic field(Blandford-Payne) [101] may be possible.
disk
PBH jet
cocoon(shocked material)
wind
FIG. 2. Schematic diagram for PBH jet with cocoon, asso-ciated with a spinning PBH, and wind outflow emission. Thecocoon shock expands into the ISM with speeds vh along thejet-axis and vc in orthogonal directions. Mean cocoon cross-sectional area Ac, area of the tip bow shock Ah as well as jetopening angle θ0 are shown.
104], allowing for a highly efficient engine powering thejet with a luminosity
Lj = εjMacc , (5)
where εj ∼ O(1) is the jet efficiency factor [105] andMacc is the disk accretion rate given by Eq. (3). Sucha scenario is consistent with the recently imaged ring ofthe M87 galaxy central BH [106] as well as the analysisof blazar spectral energy distribution [107] 2.
The jet interacts with external material, forming a pairof forward and reverse shocks. Then a significant O(1)portion of the jet power is deposited into an expanding“cocoon” consisting of the shocked material [111]. InFig. 3 we schematically depict the cocoon structure.
A fraction of the cocoon’s energy is radiated away asthermal bremsstrahlung emission, predominantly fromyoung cocoons as Lbrem ∼ t−1 [112]. For the scenario weconsider, the cocoons are long lived and they eventuallydeliver most of their energy efficiently to the surroundingISM (i.e., the associated system heating by the outflow isHout ∼ Min). To quantify the uncertainties, we considera range from Hout = Macc to Hout = 5× 10−3Macc. Theformer value is motivated by jets associated with MADs.The latter value, which is more conservative, is moti-vated by the AGN feedback consideration for the windalthough it may also be achieved by inefficient jets.
The cocoon can be analytically characterized usingonly the jet luminosity Lj , the density of the ambientgas medium ρa and the jet opening angle θ0 ∼few de-grees [113]. Using Eq. (2) and (3) of Ref. [111] and Eq.(12) of Ref. [113], and considering a relativistic jet prop-agation speed of vj ' 1, we obtain the cocoon sideways
2 However, extended jet studies indicate εj ∼ O(10−2) [108–110].
4
100 102 104 106 108 1010 1012 1014 1016
t (s)
10−26
10−21
10−16
10−11
10−6
10−1
104
109
1014
1019C
oco
onV
olum
e(p
c3)
FIG. 3. Cocoon volume as a function of time for a gassystem such as the Leo T dwarf galaxy. Results for PBHsof masses M=10−3M (black), 1M (red), 103M (green),and 106M (blue) are shown. For reference, the black dashedline indicates the total volume of the inner region of Leo T,1.8 × 108pc3.
expansion speed
vc ≈(Ljθ0
2ρat2
)1/5
∼ 103 km/s ε1/5j
(M
1 M
)2/5(v
10 km/s
)−3/5
×(θ0
0.1
)1/5(t
1 yr
)−2/5. (6)
Using Eq. (6) with Eq. (2) of Ref. [111], and consideringthat the jet’s mean cross-sectional area is Ac ' v2
c t2, the
speed of cocoon expansion along the jet-axis is
vh ≈Ljt
2
ρaA2c
≈( 24Ljρat2θ4
0
)1/5
∼ 2× 104 km/s ε1/5j
(M
1 M
)2/5(v
10 km/s
)−3/5
×(θ0
0.1
)−4/5(t
1 yr
)−2/5. (7)
The resulting cocoon volume is then
Vc ≈ v2cvht
3 ≈(22t9L3
j
ρ3aθ
20
)1/5
' 2.1× 10−8 pc3ε3/5j
(M
1 M
)6/5(v
10 km/s
)−9/5
×(θ0
0.1
)−2/5(t
1 yr
)9/5. (8)
The time tb it takes for the expanding cocoon width to
reach the Bondi radius is
tb ≈(
6GM5v2
)5/3( 2ρaLjθ0
)1/3
' 6.9× 10−3 yr ε−1/3j
(M
1 M
)×(
v
10 km/s
)−7/3(θ0
0.1
)−1/3. (9)
The number of PBHs of mass M contributing a frac-tion fDM of the DM abundance within a system of radiusrsys and uniform DM density ρDM is
NPBH = 43πr
3sys
(ρDMfPBH
M
)' 8.3× 106 fPBH
(rsys
350 pc
)3
×(
ρDM
1.75 GeV/cm3
)(M
1 M
)−1. (10)
Solving the equation Vsys = NPBHVc(tfill), the time tfill ittakes for the volume of PBH cocoons to fill up the volumeVsys = (4/3)πr3
sys of a system of gas is
tfill ≈(
M
ρDMfPBH
)5/9vθ
2/90
22/9(4πG2M2)1/3
∼ 105 yr f−5/9PBH
(M
1 M
)−1/9(v
10 km/s
)×(θ0
0.1
)2/9(ρDM
1.75 GeV/cm−3
)−5/9. (11)
We note that Eq. (11) is independent of the system size.Comparing Eq. (11) with Eq. (9) allows to define the
condition tb tfill such that effects of feedback willnot have any potential impact on PBH accretion dur-ing timescales tfill associated with the volume of PBHcocoons filling the system of interest, which requires
v 6× 10−2 km/s ε−1/10j f
1/6PBH
( θ0
0.1
)−1/6
×( M
1 M
)1/3(
ρDM
1.75 GeV/cm−3
)1/6. (12)
This condition is difficult to satisfy except e.g. for asmall jet opening angle θ0. Hence, the complication ef-fects associated with feedback could be in principle ofsome relevance. However, it is reasonable to expect thatefficient accretion will still persist, e.g. in the equatorialplane.
IV. WINDS
Aside from collimated jets associated with spinningPBHs, both spinning and nonspinning PBHs can natu-rally form sub-relativistic outflows of ionized gas through
5
a variety of mechanisms (e.g., [114–117]). The signifi-cance of such disk-driven winds has been recently high-lighted for nonrotating PBHs [67, 69]. There, the windswere treated employing a phenomenological self-similarmodel [90] and their energy deposit was estimated fromstopping power considerations. However, the descriptionof winds is uncertain and the winds should rather de-posit a sizable amount of energy into surrounding ma-terial via shock heating, similarly to cocoons. More so,the wind energy deposit can be efficient (e.g., [118, 119]).Hence, here we consider a simplified phenomenologicaltreatment, parametrizing the wind power analogously tothat of jets and cocoons with wind luminosity Lw givenby
Lw = εwMout , (13)
where εw is the wind efficiency factor.The ratio of power efficiencies of jets and winds is a
matter of ongoing debate (see e.g., [120] for discussion ofpossible wind-jet connections). In our subsequent discus-sion of gas heating, we assume different efficiency con-tributions of jets and winds. For the wind, motivatedby the AGN feedback consideration, we adopt Hout =5 × 10−3Macc, which implies that ∼ 5% of the quasarbolometric luminosity (that is typically ∼ 0.1Macc) isdissipated for the ISM heating [119]. We do not distin-guish between the individual wind and jet contributionsto gas heating. However, we expect that the jet contribu-tion is more significant, e.g. in case of MADs [104, 121].Observationally, jets can be distinguished from winds byanalysis of the emission morphology and the detectionof “hot spots” associated with strong shocks where jetsterminate [122]. Jet signatures from isolated BHs havebeen studied in Ref. [123].
V. GAS HEATING
The deposition of energy by PBHs into the ISM heatsthe surrounding gas. Analyses of stellar and intermediatemass Schwarzschild PBHs [67, 69] as well as evaporatingPBHs [86, 131] demonstrated that considerations basedon balancing gas heating and cooling within a target sys-tem is a powerful method for exploring and constrainingPBHs3, considering particularly favorable environmentssuch as the DM-rich Leo T dwarf galaxy. Using the re-sults obtained above, we now discuss gas heating in LeoT due to PBHs. Our analysis can be readily applied toother systems.
PBHs heat the gas system by a total amount Htot =NPBHH(M) = fPBHρDMVsysH(M)/M , where H(M) isthe average heat generated by one PBH of mass M
3 Our approach to set the limits is similar to that used for particleDM [132–134], but the heating mechanisms and the preferred gassystems are different in our case.
10−5 10−3 10−1 101 103 105 107
M (M)
10−7
10−6
10−5
10−4
10−3
10−2
10−1
100
f DM
P
XRB
DF
I
E
Ly-α
S
LSS
X/RO
GW
high eff.
low eff.
FIG. 4. Constraints from PBH gas heating of the Leo Tdwarf galaxy. Effects of jets and winds are shown with blackhatching over a broad range betweenHout = Macc (“high eff.”)and Hout = 5×10−3Macc (“low eff.”), assuming all PBHs formefficient jets and winds (black dashed) or that only 50% do(black dot-dashed). Gas heating contributions from disk emis-sion and dynamical friction are shown in blue and of spinningPBHs in black (see text). These constraints are bounded bythe PBH incredulity limit (positive slope line). Other existingconstraints (see Ref. [32]) are shown by dashed lines includ-ing Icarus [124] (I) caustic crossing in purple, Planck [62, 68](P) in yellow, X-ray binaries [63] (XRB) in green, dynamicalfriction of halo objects (DF) in red, Lyman-α [125] (Ly-α) inmaroon, combined bounds from the survival of astrophysicalsystems in Eridanus II [126], Segue 1 [127], and disruption ofwide binaries [128] (S) shown in magenta, large scale struc-ture [25] (LSS) in cyan, X-ray/radio [129] (X/R) in brown,and gravitational waves (GWs) in green [130].
through the different contributions. Requiring the to-tal heating not to exceed the total cooling CVsys of thesystem, where Vsys is the relevant volume of interest andC is the cooling rate, the PBH DM abundance fPBH isconstrained by
fPBH < fbound = MC
ρDMH(M) (14)
' 6× 10−5(
M
1 M
)(C
2.28× 10−30 erg/(cm3 s)
)×(
ρDM
1.75 GeV/cm−3
)−1(H(M)
2.3× 1031 erg/s
)−1,
where the inserted quantities are characteristic of Leo Twith H(M) being efficient jet heating.
We consider gas heating due to the combined contribu-tions of accretion disk emission Eq. (4), dynamical fric-tion Fdyn, and outflows associated with jets and windswhose heating rate is Hout ' Lj + Lw. For the system,we limit our considerations to the central r . 350 pcregion of Leo T, which is dominated by atomic hydro-
6
gen4 [135]. For the varying central gas density we takethe approximate constant value n = 0.07 cm−3 [135]and ρDM = 1.75 GeV/cm3. Focusing on the domi-nant gas component, we consider a velocity dispersion ofσg = 6.9 km/s and a temperature T ' 6000 K [135, 137].Since the DM is expected to have the same velocity dis-persion as the gas, we set σv = σg. From the adiabaticformula with input temperature of T ' 6000 K we de-termine the sound speed to be cs = 9 km/s. Combin-ing the radius and number density, we obtain the col-umn density of hydrogen gas in the central region of LeoT is nrsys = 7.56 × 1019 cm−2. For the gas metallicitywe consider that it approximately follows the stellar one[Fe/H] ' −2 estimated from the stellar spectra [138],which is accurate up to a factor of few.
For the system cooling rate, we employ the approxi-mate results of Ref. [134]. For hydrogen gas it is
C =( n
1 cm−3
)210[Fe/H]Λ(T ) erg
cm3s , (15)
where [Fe/H] ≡ log10(nFe/nH)gas − log10(nFe/nH)Sun isthe metallicity, and Λ(T ) ∝ 10[Fe/H] is the cooling func-tion. Fitting numerically results of the chemical net-work library [136], one can obtain that Λ(T ) = 2.51 ×10−28(T/K)0.6 is valid for 300 K < T < 8000 K [134].For Leo T, 10[Fe/H] ' 10−2.
Conservatively, we neglect possible additional heatingcontributions from natural sources such as stellar radi-ation. Further, we ensure that the system is stable byrequiring that its lifetime τsys significantly exceeds thethermalization timescale ttherm, given by
ttherm = 32nkT
C(16)
' 1.2× 109 yr(
T
6000 K
)×( n
0.07 cm−3
)( C
2.28× 10−30 erg/(cm3 s)
)−1
,
where k is the Boltzmann constant. A time for cocoonsto fill the system shorter than ttherm ensures a continuousheating/cooling process. Comparing Eq. (11) to Eq. (16),tfill ttherm implies
fPBH > 5.2× 10−8(
v
10 km/s
)9/5(M
1 M
)−1/5
×(
ρDM
1.75 GeV/cm3
)−1 ( n
0.07 cm−3
)−9/5θ
2/50
×(
C
2.21× 10−30 erg/(cm3 s)
)9/5(T
6000 K
)−9/5.
(17)
4 The gas outside is expected to be ionized [135], resulting in effi-cient cooling [136].
This condition does not impact our limits because theyare more stringent.
PBH effects are relevant only if statistically there isat least one PBH within the considered system, i.e. iffPBH ρDM(4πr3
sys/3)/M > 1. This establishes the in-credulity limit. Hence, we restrict our constraints to
fPBH >3M
4πr3sysρDM
. (18)
In Fig. 4 we display the resulting limits from gas heat-ing in Leo T on PBHs contributing to the DM, along withother existing constraints. The constraints we found dueto PBH outflows (jets or winds), are shown in the hatchedblack regions. The dashed lines correspond to differ-ent contributions Hout to the heating rate, Hout = Macc(“high eff.”) corresponds to jets associated with highlyefficient magnetically arrested disks, while the conserva-tive Hout = 5 × 10−3Macc (“low eff.”) is suggested byAGN feedback for disk-winds. All intermediate Hout arealso possible. Jets and winds can act as sensitive probesof PBH parameter space and stringent constraints can beplaced by PBH jets.
VI. CONCLUSIONS
PBHs formed in the early Universe can contribute afraction or all of the DM abundance and have been di-rectly linked with GW and other observations. We havestudied for the first time the energy deposition and con-tributions to ISM gas heating from jets with cocoons as-sociated with spinning PBHs as well as outflowing winds.We have demonstrated that these combined outflow ef-fects can act as sensitive probes of PBHs over orders ofmagnitude in mass range, from ∼ 10−2M to 106M.This range is particularly of interest for LIGO/VIRGOGW events. The robustness and strength of our resultsis further established for spinning PBHs, which can sus-tain highly efficient relativistic jets in addition to windsas a separate powerful emission source. Contributions ofjets and winds can be discriminated by analysis of theemission morphology as well as the detection of jet hotspots, allowing the potential for indirect insights into thespin distribution (and hence formation models) of PBHs.
ACKNOWLEDGMENTS
We thank Kunihito Ioka for discussion. The workof G.B.G. and P.L. was supported in part by theU.S. Department of Energy (DOE) Grant No. DE-SC0009937. P.L is also supported by Grant Korea NRF-2019R1C1C1010050. The work of K.M. is supportedby the NSF Grant No. AST-1908689, No. AST-2108466and No. AST-2108467, and KAKENHI No. 20H01901
7
and No. 20H05852. The work of Y.I. is supported byJSPS KAKENHI grant No. JP18H05458, JP19K14772,program of Leading Initiative for Excellent Young Re-searchers, MEXT, Japan, and RIKEN iTHEMS Pro-gram. V.T., and Y.I. are also supported by the World
Premier International Research Center Initiative (WPI),MEXT, Japan. This work was performed in part at theAspen Center for Physics, which is supported by NationalScience Foundation grant PHY-1607611.
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